Toward a Deterministic Model of Planetary Formation. III. Mass Distribution of Short-Period Planets around Stars of Various Masses

By Shigeru Ida, D. Lin. 2005

404 citations recorded by the source corpus.

The origin of a recently discovered close-in Neptune-mass planet around GJ 436 poses a challenge to the current theories of planet formation. On the basis of the sequential accretion hypothesis and the standard theory of gap formation and orbital migration, we show that around M dwarf stars, close-in Neptune-mass ice giant planets may be relatively common, while close-in Jupiter-mass gas giant planets are relatively rare. The mass distribution of close-in planets generally has two peaks at about Neptune mass and Jupiter mass. The lower mass peak takes the maximum frequency for M dwarfs. Around more massive solar-type stars (G dwarfs), the higher mass peak is much more pronounced. Planets around G dwarfs undergo orbital migration after fully accreting gas, while those around M dwarfs tend to migrate before starting rapid gas accretion. Close-in Neptune-mass planets may also exist around G dwarfs, although they tend to be mostly composed of silicates and iron cores and their frequency is expected to be much smaller than that of Neptune-mass planets around M dwarfs and that of gas giants around G dwarfs. We also show that the conditions for planets' migration due to their tidal interaction with the disk and the stellar mass dependence in the disk mass distribution can be calibrated by the mass distribution of short-period planets around host stars with various masses.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/39baf74bc71927aacce760c49762b1980a340bec

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Citations in the corpus

The HARPS search for southern extra-solar planets - XXXI. The M-dwarf sample (2011, background): “The mass of the proto-planetary disk, its temperature and density profiles, gravity, the gas-dissipation timescale, etc... all change with stellar mass (e.g. Ida & Lin 2005).”
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Planet Formation around Stars of Various Masses: The Snow Line and the Frequency of Giant Planets (2007, methodology): “The width of the regions where cores form increases with stellar mass (Figure 4, Ida & Lin 2005).”
THE NIRSPEC ULTRACOOL DWARF RADIAL VELOCITY SURVEY (2010, background): “A significant population of giant planets orbiting close to M and L dwarfs is not predicted by models of planet formation via core accretion (i.e., Laughlin et al. 2004; Ida & Lin 2005), though such planets may be formed in the disk instability scenario (Boss 2006).”
KEPLER PLANETS: A TALE OF EVAPORATION (2013, background): “It is at this point that we will begin to learn valuable information about the planet population at birth and make inferences about the planet formation process (e.g Ida & Lin 2005; Mordasini et al. 2012a,b; Hansen & Murray 2012, 2013).”
THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS (2013, background): “…and stellar host mass (M∗) noted by Johnson et al. (2007), which was predicted theoretically in planet formation models that implicitly assumed there is a fundamental scaling relationship between Md and M∗ (e.g., Laughlin et al. 2004; Ida & Lin 2005; Kornet et al. 2006; Alibert et al. 2011).”
PLANETARY POPULATION SYNTHESIS COUPLED WITH ATMOSPHERIC ESCAPE: A STATISTICAL VIEW OF EVAPORATION (2014, background): “K/M-dwarfs are predicted to yield more Neptunian planets but fewer Jovian planets (Ida & Lin 2005; Alibert et al. 2011).”
Precise Radial Velocities of Giant Stars VII. Occurrence Rate of Giant Extrasolar Planets as a Function of Mass and Metallicity (2014, background): “A strong decrease in planet occurrence rates for stellar masses above roughly 1.5 to 3 M is predicted in the semianalytic planet formations models by Ida & Lin (2005) and Kennedy & Kenyon (2008a).”
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Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog (2006, methodology): “Using extensive numerical simulations, Ida & Lin (2005) derived a positive correlation between the characteristic planetary mass and the stellar mass within the range 0.2 – 1.5M⊙.”
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Extrasolar planets and brown dwarfs around A-F type stars. VI. High precision RV survey of early type dwarfs with HARPS (2008, background): “There are theoretical indications that the mass of the planets increases with the mass of the parent star, at least for low-mass stars (Ida & Lin 2005) and that the frequency of giant planets increases linearly with the parent-star mass for stars between 0.4 and 3 M (Kennedy & Kenyon 2008), with…”